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The Application database is the archived database; “Science” data, binned in time and frequency for use by the Data Analysis SW - in MIRIAD format (can also do FITS format if people want to use non-MIRIAD SW). We expect at least three types of datasets, magnetography, bursts, and utility.

The File database is a set of files containing information about the time range covered by each Application dataset.

(Not sure if it’s possible to create an event list in an automated process, will start with RHESSI-like process.)

Partial calibration happens in the DPP process, the data are calibrated using a time-independent gain factors. It is expected that this will be useful for simple tasks like spectral generation, but not for maps.

The L0 process will analyze calibrator data, then apply or add time-dependent calibration. Post-imaging, more calibration might occur (maybe from “self-cal” or “closure phase output”) and added back into the ADB.

Once we have good calibrations, we can make maps of the Sun. Given a flare list, we can create flare images in some standard frequency bands. Also we will image active regions. Full Sun imaging may also be an option.

Once the “Process” button is clicked, the IDL program generates a series of MIRIAD commands, which are written to a file.

If the user has MIRIAD on his system, a process is spawned, and maps are created.

If the user has no MIRIAD, then there is an option to upload the command file to our server, which will queue and then run the process. The user can choose to be notified via email that his process has been run, or the IDL shell can be configured to automatically look for results.

Image maps are saved in (FITS, MIRIAD or FITS or both) format. The EOVSA program will be able to read and display the image files.